Astronomy:Long Period Radio Transients

From HandWiki
Short description: New class of galactic astronomical transients - LPTs


Long-period radio transients (LPTs) are a class of Galactic radio sources that emit highly polarised, coherent bursts of radio emission that regularly repeat, with periods ranging few minutes to several hours. Unlike classical pulsars, which are neutron stars that rotate on timescales of milliseconds to seconds, LPTs have periods orders of magnitude longer — often exceeding conventional theoretical limits for radio-emitting neutron stars[1]. Their physical nature remains actively debated, with the hypotheses suggesting either slowly rotating magnetars or white dwarf–red dwarf binary systems, though isolated magnetic white dwarfs have been suggested as well.

The first hint of such a phenomenon was the detection of GCRT J1745−3009 near the Galactic Centre in 2005 [2]. Since 2022 there has been a wave of discoveries, driven by wide-field radio telescopes such as the Murchison Widefield Array (MWA) and the Australian SKA Pathfinder (ASKAP), which have established LPTs as a distinct and growing class of astrophysical object. As of 2026, roughly 12 confirmed LPTs are known[3], and dedicated surveys continue to expand the sample.

Characteristics

LPTs are defined by several observational properties that distinguish them from other known radio transients:

  • Periods of minutes to hours — far longer than those of ordinary pulsars or millisecond pulsars (milliseconds to seconds).
  • Highly polarised radio pulses — linear polarisation fractions commonly exceeding 70–90%, with circular fractions reaching 20–30%, consistent with coherent emission mechanisms such as those seen in canonical pulsars and repeating fast radio bursts (FRBs).
  • Pulse durations of from seconds to tens of minutes, yielding duty cycles that can be quite large.
  • Brightness temperatures far exceeding 1012 K, implying a coherent emission mechanism, and possible relativistic magnetised plasmas.
  • Concentration toward the Galactic plane, though some sources are found at high Galactic latitudes.
  • Emission activity that can be transient (lasting weeks to months) or persistent over decades, depending on the source.

Some LPTs exhibit emission-state switching — alternating between bright pulses, faint pulses, and quiescence — analogous to mode-changing behaviour in radio pulsars and magnetars. Notably, ASKAP J1935+2148 displays several distinct emission modes despite its 54-minute period[4]. Some sources also show complex polarisation position angle swings consistent with the rotating vector models used for pulsars.

Discovery history

Precursor: GCRT J1745−3009 (2005)

The earliest candidate LPT, GCRT J1745−3009, was detected by Hyman et al. in 2005[2] using archival Very Large Array (VLA) data at 330 MHz. It produced five bursts of roughly equal brightness, each lasting about 10 minutes, recurring every 77 minutes during a 7-hour window on 30 September – 1 October 2002. Its extremely high inferred brightness temperature (~1016 K if near the Galactic Centre) and morphology were unlike any known class of radio transient at the time, and it was provisionally categorised as a Galactic Center Radio Transient (GCRT). Its classification as an LPT remains debated owing to the lack of subsequent detections and uncertainty about its distance.

Modern era (2022–present)

The modern LPT era began in 2022 when Hurley-Walker et al.[5] reported GLEAM-X J162759.5−523504.3 using the Murchison Widefield Array, with a period of approximately 18 minutes. The source emitted highly polarised pulses for several months before becoming quiescent. That same year, Caleb et al.[6] discovered a new long-period pulsar, using the MeerKAT radio telescope, with a 76 second spin period. In 2023, Hurley-Walker et al. discovered GPM J1839−10, which has a 21-minute pulsation period and was subsequently found to have been active for at least 35 years through archival searches extending back to 1988 — making it the longest-lived known LPT[7].

From 2024 onward, the discovery rate accelerated significantly, driven by increasing wide-field surveys with ASKAP, LOFAR, and CHIME. Notable additions include ASKAP J1935+2148 (54-minute period)[4], ASKAP J1832−0911 (which has also been detected in X-rays)[8] , and several other systems suspected to binary systems containing white dwarf with an M-dwarf companion [9][10].

Known sources

As of mid-2026, 12 LPTs have been confirmed. Two binary-system LPTs with orbital periods between 2.1 hours and 2.9 hours are established, along with 10 apparently isolated LPTs with periods from 14 minutes to 6.5 hours.[3]

Known long-period radio transients
Source Period Discovery year Facility Notes
GCRT J1745−3009 77.01 min 2005 VLA Probable precursor; Galactic Centre direction; classification debated
GLEAM-X J162759.5−523504.3 18.18 min 2022 MWA Active for ~3 months; first modern LPT
GPM J1839−10 21.97 min 2023 MWA Active since at least 1988; 9-hour binary orbit
ASKAP J1935+2148 53.76 min 2024 ASKAP Multiple emission states
ASKAP / DART J1832−0911 44.27 min 2024 ASKAP / DART Only known LPT with periodic X-ray; no optical counterpart
ILT J1101+5521 125.53 min 2024 LOFAR Confirmed binary; optical spectrum consistent with M-dwarf [9]
GLEAM-X J0704−37 174.94 min 2024 MWA Confirmed binary; optical spectrum consistent with M-dwarf
ASKAP J1839-0756 387.02 min 2025 ASKAP Longest known period (~6.45 hr); exhibits weak interpulse emission at half-period
ASKAP J1448-6857 93.85 min 2025 ASKAP Detected at X-ray wavelengths; no confirmed X-ray period[11]
CHIME / ILT J163430+445010 14.02 min 2025 LOFAR / CHIME ~100% circularly polarised; no optical counterpart [12] [13]
ASKAP J1755-2527 69.77 min 2024 ASKAP Intermittent; discovered as a single pulse; switched back on months later [14] [15]
ASKAP J142431.2-612611 35.79 min 2026 ASKAP Intermittent; only observed for a few weeks[16]

Theoretical models

No single model has achieved consensus in explaining all observed LPTs. Several competing hypotheses are actively considered.

Ultra-slowly rotating magnetar

The most widely discussed model invokes a neutron star with an extremely strong magnetic field (a magnetar) that has spun down to rotation periods of minutes or more, possibly aided by fallback accretion from supernova ejecta shortly after birth [17]. Magnetars are known to emit coherent, highly polarised radio pulses, and LPT characteristics — including mode switching and polarisation behaviour — qualitatively resemble magnetar phenomenology. However, most LPT periods place the sources in or beyond the classical pulsar "death valley" — the region of period-period derivative diagram|period–period-derivative (P–Ṗ) phase space where pair production in the magnetosphere should cease, shutting off coherent radio emission. Whether alternative magnetic field configurations (twisted or multipolar fields) can sustain emission across this boundary is an open theoretical question.

Magnetic white dwarf

Some LPTs may be rapidly rotating (on astronomical timescales) magnetic white dwarfs producing coherent radio emission via electron cyclotron maser instability or similar processes. Pulsating white dwarf systems are known to emit radio waves — AR Scorpii being a prominent example — and the period range of LPTs is physically plausible for white dwarf spins and/or orbits. This model naturally explains sources found in binaries, and is supported by multi-wavelength detections of optical counterparts that hint at white dwarf companions to M-dwarfs. To date there has not been a radio detection of an isolated white dwarf, making the pulsating white dwarf a somewhat speculative hypothesis.

White dwarf binary interaction

For a subset of LPTs now confirmed to be in binary systems (e.g., ILT J1101+5521[9], GLEAM-X J0704−37[10]), the observed radio periodicity matches the orbital period rather than a spin period. In this framework, the white dwarf's magnetic field interacts with a companion star (typically an M-dwarf or ultracool dwarf), inducing coherent radio emission — analogous to Jupiter–Io magnetospheric interactions but on a stellar scale. GPM J1839−10, the longest-lived LPT, has itself been found to have a 9-hour binary orbit, linking it observationally to white dwarf pulsar systems.[18]

Other hypotheses

Additional theoretical proposals include precessing neutron star–black hole binaries producing apparent ultra-long periods through self-lensing, and hypothetical objects composed of strange quark matter ("strange dwarf pulsars"). These models remain speculative and lack direct observational support.

Observational facilities

LPTs operate on timescales that fall in a historically under-explored gap between fast radio transients (milliseconds) and slow synchrotron variables (days to months). Their detection has been enabled by a new generation of wide-field radio interferometers capable of imaging at cadences of seconds to minutes:

  • Murchison Widefield Array (MWA), Western Australia — site of the first modern LPT discoveries.
  • Australian SKA Pathfinder (ASKAP) — Western Australia, enabled sensitive, wide-field surveys at gigahertz frequencies.
  • Low-Frequency Array (LOFAR), Europe — has contributed discoveries at low radio frequencies, including high-declination sources.
  • MeerKAT, South Africa — used for sensitive targeted follow-up and discovery.
  • Canadian Hydrogen Intensity Mapping Experiment (CHIME) — contributed to finding LPTs with timing solutions, including a source exhibiting a timing glitch.

Multi-wavelength follow-up observations with X-ray telescopes (e.g., Swift, XMM-Newton, Chandra) and optical telescopes have been critical in identifying binary companions and constraining the physical nature of individual sources.

Significance and open questions

Long-period radio transients challenge established models of neutron star evolution and pulsar emission. Their existence in the period–period-derivative diagram near or beyond the pulsar death valley suggests that either the death-line theories require revision[1], or that at least some LPTs belong to a fundamentally different class of object than rotation-powered neutron stars.

Key open questions include:

  • What fraction of LPTs are neutron stars versus white dwarfs?
  • How do LPTs maintain coherent emission at such long rotation periods?
  • What is the relationship between apparently isolated LPTs and binary-system LPTs?
  • Are Galactic Center Radio Transients (GCRTs) the same phenomenon as modern LPTs?
  • How large is the total Galactic LPT population, and what are the selection biases of current surveys?

The rapid pace of discovery since 2022 suggests that the LPT population may be substantially larger than currently sampled. Future surveys with the Square Kilometre Array (SKA) and its precursors are expected to dramatically expand the known census.

See also

References

  1. ↑ 1.0 1.1 Rea, N. (2024). "Long-period Radio Pulsars: Population Study in the Neutron Star and White Dwarf Rotating Dipole Scenarios". The Astrophysical Journal Letters 961 (2): 214. doi:10.3847/1538-4357/ad165d. Bibcode: 2024ApJ...961..214R. 
  2. ↑ 2.0 2.1 Hyman, S. D.; Lazio, T. J. W.; Kassim, N. E.; Ray, P. S.; Markwardt, C. B.; Yusef-Zadeh, F. (2005). "A powerful bursting radio source towards the Galactic Centre". Nature 434 (7029): 50–52. doi:10.1038/nature03400. PMID 15744294. Bibcode: 2005Natur.434...50H. 
  3. ↑ 3.0 3.1 Rea, N. (2026). "Long Period Transients (LPTs): a comprehensive review". Journal of High Energy Astrophysics 52. doi:10.1016/j.jheap.2026.100566. Bibcode: 2026JHEAp..5200566R. 
  4. ↑ 4.0 4.1 Caleb, M. (2024). "An emission-state-switching radio transient with a 54-minute period". Nature Astronomy 8 (9): 1159–1168. doi:10.1038/s41550-024-02277-w. Bibcode: 2024NatAs...8.1159C. 
  5. ↑ Hurley-Walker, N. (2022). "A radio transient with unusually slow periodic emission". Nature 601 (7894): 526–530. doi:10.1038/s41586-021-04272-x. PMID 35082416. Bibcode: 2022Natur.601..526H. 
  6. ↑ Caleb, M. (2022). "Discovery of a radio-emitting neutron star with an ultra-long spin period of 76 s". Nature Astronomy 6 (7): 828–836. doi:10.1038/s41550-022-01688-x. PMID 35880202. Bibcode: 2022NatAs...6..828C. 
  7. ↑ Hurley-Walker, N. (2023). "A long-period radio transient active for three decades". Nature 619 (7970): 487–490. doi:10.1038/s41586-023-06202-5. PMID 37468588. Bibcode: 2023Natur.619..487H. 
  8. ↑ Wang, Z. (2024). "Detection of X-ray Emission from a Bright Long-Period Radio Transient". Nature 642 (8068): 583–586. doi:10.1038/s41586-025-09077-w. PMID 40437090. 
  9. ↑ 9.0 9.1 9.2 de Ruiter, I. (2024). "A long-period radio transient in a binary system". Nature Astronomy. doi:10.1038/s41550-025-02491-0. 
  10. ↑ 10.0 10.1 Hurley-Walker, N. (2024). "A 2.9 hr Periodic Radio Transient with an Optical Counterpart". The Astrophysical Journal Letters 976 (2): L21. doi:10.3847/2041-8213/ad890e. Bibcode: 2024ApJ...976L..21H. 
  11. ↑ Anumarlapudi, A. (2025). "ASKAP J144834−685644: a newly discovered long period radio transient detected from radio to X-rays". Monthly Notices of the Royal Astronomical Society 542 (2): 1208–1232. doi:10.1093/mnras/staf1227. 
  12. ↑ Dong, F. A. (2025). "CHIME/FRB/Pulsar discovery of a nearby long-period radio transient with a timing glitch". The Astrophysical Journal Letters 990: L49. doi:10.3847/2041-8213/adfa8e. 
  13. ↑ Bloot, S. (2025). "Strongly polarised radio pulses from a new white-dwarf-hosting long-period transient". Astronomy & Astrophysics 699: A341. doi:10.1051/0004-6361/202555131. Bibcode: 2025A&A...699A.341B. 
  14. ↑ Dobie, D. (2024). "A two-minute burst of highly polarized radio emission originating from low Galactic latitude". Monthly Notices of the Royal Astronomical Society 535: 909–923. doi:10.1093/mnras/stae2376. 
  15. ↑ McSweeney, S. (2025). "A new long-period radio transient: discovery of pulses repeating every 1.16 h from ASKAP J175534.9−252749.1". Monthly Notices of the Royal Astronomical Society 542: 203–214. doi:10.1093/mnras/staf1203. 
  16. ↑ Pritchard, J. (2026). "Discovery of a 36-minute long-period transient ASKAP J142431.2-612611". Publications of the Astronomical Society of Australia. 
  17. ↑ Beniamini, P. (2020). "Periodicity in recurrent fast radio bursts and the origin of ultralong period magnetars". Monthly Notices of the Royal Astronomical Society 496 (3): 3390–3401. doi:10.1093/mnras/staa1783. 
  18. ↑ Horvath, C. (2026). "A binary model of long-period radio transients and white dwarf pulsars". Nature Astronomy 10 (4): 522–530. doi:10.1038/s41550-025-02760-y. Bibcode: 2026NatAs..10..522H. 

Template:Neutron stars



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Long_Period_Radio_Transients&oldid=4387803"